Submillimeter-wave and millimeter-wave observations of the interaction of supernova remnants with molecular clouds

Details Submillimeter-wave and millimeter-wave observations of the interaction of supernova remnants with molecular clouds Submillimeter-wave and millimeter-wave observations of the interaction of supernova remnants with molecular clouds

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..556..382t&link_type=abstract

EXPLOSIVE PHENOMENA IN ASTROPHYSICAL COMPACT OBJECTS: First KIAS Astrophysics Workshop. AIP Conference Proceedings, Volume 556,

Astronomy and Astrophysics

Astrophysics

Interstellar Medium And Nebulae In Milky Way, Astronomical Observations

Scientific paper

We report on submillimeter-wave and millimeter-wave observations toward supernova remnants (SNRs) by using the James Clerk Maxwell Telescope, the Mt. Fuji submillimeter-wave telescope, and the Nobeyama 45-m radio telescope. For the supernova remnant W28, which is an EGRET gamma-ray source, we have convincingly detected the broad CO, HCO+, HCN, and SiO emission lines from the shock-accelerated gas due to the SNR-cloud interaction. The previously-reported 1720-MHz OH maser spot is found to be located at the shock front. By using the Mt. Fuji submillimeter-wave telescope, we observed the 492-GHz CI (neutral atomic carbon), 345-GHz CO (3-2) and 330-GHz 13CO (3-2) emission toward SNRs, W44 and W51B/C. We found that the CI/CO and CI/13CO intensity ratio tends to be high in the SNR-cloud interaction region in W51B/C SNR. This fact might suggest the CI relative abundance is enhanced by the interaction, not only in the SNR IC 443, but also in W51B/C SNR. .

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